which relies on both the stellar surface magnetic field strength and
on the stellar rotation velocity \(v_{\rm rot}\) . This so-called Parker
stellar wind is a parametrisation for magnetised low-mass stars which
has been developed and widely-used in studies devoted to the
heliosphere [1]}, [2]}, [3]}, [4]}.
It has been adapted to the intermediate stellar mass regime in
works investigating the shaping of planetary nebula [5]}, [6]}, [7]}, [8]}
and stellar wind bow shocks [9]}, [10]}, [11]}, respectively.
